[29.12] Core Kinematics in the Starburst-Ring Sab Galaxy NGC 4736

NGC 4736 (M94) is notable as the nearest early-type spiral
galaxy of low inclination, and as the nearest example of a
starbursting resonance-ring system. Interior to its inner
star-forming ring is a luminous core containing a mix of old
red stars and young UV-bright stars. Early long-slit
spectroscopy revealed unusually high rotation speeds
relative to the velocity dispersions, prompting Kormendy
(1982) to describe the core as the innermost part of the
disk, rather than the densest part of the spheroid (ie. the
classic ``bulge''). Using the WIYN 3.5-m telescope, DensePak
fiber array, and Bench spectrograph, we have carried out
integral field spectroscopy of the central 45'' \times
30'' (1.0 kpc \times 0.7 kpc) in M94. Our kinematic
mapping confirms the earlier claims of high rotation
velocities relative to the velocity dispersions. Rotation
curves of the stars and CO gas (from a recent
interferometric mapping by Wong and Blitz [2000]) show the
stars rotating slower by ~20--35 km/sec relative to the
gas. Plans for analyzing the stellar kinematics as a
function of stellar type (and corresponding age) are
described.